用CANDELS约束正规和紧致被动演化Galerkin系统从红移z=3到现在的装配
Constraining The Assembly Of Normal And Compact Passively Evolving Galaxies From Redshift z=3 To The Present With CANDELS
摘要：
我们利用GOODS-South领域的独特数据集，包括最近获得的作为宇宙组装近红外深河外遗留巡天（CANDELS）一部分的WFC 3图像，研究了从z~3到z~1的具有广泛恒星质量范围（10^10<M*/Msun<10^11.5）的被动早型星系的数密度演化，作为大小的函数。特别是，我们选择了107个大质量（M*> 10 ^10 M_sun）、被动（SSFR<10^-2 Gyr^-1）和1.2<z<3的形态学球状星系的样本，利用了GOODS可用的全色数据集，包括VLT、CFHT、斯皮策、钱德拉和HST ACS+ WFC 3数据。我们发现，在1<z<3时，被动演化的早期型星系是宇宙中最红、质量最大的天体，我们证明了质量、形态、颜色和恒星形成活动之间的相关性在那个时期已经存在。我们测量了被动早型星系（ETG）的质量-尺寸关系从z~3到z~1的显著演化，星系的尺寸仅在3 Gyr时间尺度内平均增长2倍。我们还见证了被动ETG的数量密度在同一时间间隔内增加了50倍。我们发现，在z>2时形成的第一个ETG都是紧凑或超紧凑的，而正常尺寸的ETG（即尺寸与相同质量的局部对应物相当的ETG）仅在z<1时是最常见的ETG。在0<z<1处ETG平均尺寸的增加主要是由新的大ETG的出现而不是由单个星系的尺寸增加驱动的。
英文摘要：
We study the evolution of the number density, as a function of the size, of passive early-type galaxies with a wide range of stellar masses 10^10<M*/Msun<10^11.5) from z~3 to z~1, exploiting the unique dataset available in the GOODS-South field, including the recently obtained WFC3 images as a part of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS). In particular, we select a sample of 107 massive (M*>10^10 M_sun), passive (SSFR<10^-2 Gyr^-1) and morphologically spheroidal galaxies at 1.2<z<3, taking advantage of the panchromatic dataset available for GOODS, including VLT, CFHT, Spitzer, Chandra and HST ACS+WFC3 data. We find that at 1<z<3 the passively evolving early-type galaxies are the reddest and most massive objects in the Universe, and we prove that a correlation between mass, morphology, color and star-formation activity is already in place at that epoch. We measure a significant evolution in the mass-size relation of passive early-type galaxies (ETGs) from z~3 to z~1, with galaxies growing on average by a factor of 2 in size in a 3 Gyr timescale only. We witness also an increase in the number density of passive ETGs of 50 times over the same time interval. We find that the first ETGs to form at z>2 are all compact or ultra-compact, while normal sized ETGs (meaning ETGs with sizes comparable to those of local counterparts of the same mass) are the most common ETGs only at z<1. The increase of the average size of ETGs at 0<z<1 is primarily driven by the appearance of new large ETGs rather than by the size increase of individual galaxies.
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